Measuring cosmic bulk flows with Type Ia supernovae from the Nearby Supernova Factory (Corrigendum)

U. Feindt; M. Kerschhaggl; M. Kowalski; G. Aldering; P. Antilogus; C. Aragon; S. Bailey; C. Baltay; S. Bongard; C. Buton; A. Canto; F. Cellier-Holzem; M. Childress; N. Chotard; Y. Copin; H. K. Fakhouri; E. Gangler; J. Guy; A. Kim; P. Nugent; J. Nordin; K. Paech; R. Pain; E. Pecontal; R. Pereira; S. Perlmutter; D. Rabinowitz; M. Rigault; K. Runge; C. Saunders; R. Scalzo; G. Smadja; C. Tao; R. C. Thomas; B. A. Weaver; C. Wu

doi:10.1051/0004-6361/201321880e

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Erratum

This article is an erratum for:
[https://doi.org/10.1051/0004-6361/201321880]

Issue		A&A Volume 578, June 2015


Article Number		C1
Number of page(s)		2
Section		Cosmology (including clusters of galaxies)
DOI		https://doi.org/10.1051/0004-6361/201321880e
Published online		29 May 2015

A&A 578, C1 (2015)

Measuring cosmic bulk flows with Type Ia supernovae from the Nearby Supernova Factory (Corrigendum)

U. Feindt¹^,2, M. Kerschhaggl², M. Kowalski¹, G. Aldering³, P. Antilogus⁴, C. Aragon³, S. Bailey³, C. Baltay⁵, S. Bongard⁴, C. Buton², A. Canto⁴, F. Cellier-Holzem⁴, M. Childress⁶, N. Chotard⁷^,8, Y. Copin⁷^,8, H. K. Fakhouri³^,9, E. Gangler⁷, J. Guy⁴, A. Kim³, P. Nugent¹⁰^,11, J. Nordin¹, K. Paech², R. Pain⁴, E. Pecontal¹², R. Pereira⁷, S. Perlmutter³^,8, D. Rabinowitz⁵, M. Rigault¹, K. Runge³, C. Saunders³, R. Scalzo⁶, G. Smadja⁷, C. Tao¹³^,14, R. C. Thomas⁹, B. A. Weaver¹⁵ and C. Wu⁴^,16

¹ Institut für Physik, Humboldt-Universität zu Berlin, Newtonstraße 15, 12489 Berlin, Germany
e-mail: feindt@physik.hu-berlin.de
² Physikalisches Institut, Universität Bonn, Nußallee 12, 53115 Bonn, Germany
e-mail: mkersch@physik.uni-bonn.de
³ Physics Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94720, USA
⁴ Laboratoire de Physique Nucléaire et des Hautes Énergies, Université Pierre et Marie Curie Paris 6, Université Paris Diderot Paris 7, CNRS-IN2P3, 4 place Jussieu, 75252 Paris Cedex 05, France
⁵ Department of Physics, Yale University, New Haven, CT 06250-8121, USA
⁶ Research School of Astronomy and Astrophysics, Australian National University, Canberra, ACT 2611, Australia
⁷ Université de Lyon, 69622 Lyon, France
⁸ Université de Lyon 1, Villeurbanne, CNRS/IN2P3, Institut de Physique Nucléaire de Lyon, 69622 Lyon, France
⁹ Department of Physics, University of California Berkeley, 366 LeConte Hall MC 7300, Berkeley, CA 94720-7300, USA
¹⁰ Computational Cosmology Center, Computational Research Division, Lawrence Berkeley National Laboratory, 1 Cyclotron Road MS 50B-4206, Berkeley, CA 94720, USA
¹¹ Department of Astronomy, B-20 Hearst Field Annex # 3411, University of California, Berkeley, CA 94720-3411, USA
¹² Centre de Recherche Astronomique de Lyon, Université Lyon 1, 9 avenue Charles André, 69561 Saint Genis Laval Cedex, France
¹³ Centre de Physique des Particules de Marseille, 163, avenue de Luminy, Case 902, 13288 Marseille Cedex 09, France
¹⁴ Tsinghua Center for Astrophysics, Tsinghua University, 100084 Beijing, PR China
¹⁵ Center for Cosmology and Particle Physics, New York University, 4 Washington Place, New York, NY 10003, USA
¹⁶ National Astronomical Observatories, Chinese Academy of Sciences, 100012 Beijing, PR China

Key words: cosmology: observations / cosmological parameters / large-scale structure of Universe / supernovae: general / errata, addenda

Erratum for: A&A 560, A90 (2013), DOI: 10.1051/0004-6361/201321880

In Table 1 of Feindt et al. (2013), the p-values for the dipole fit method were calculated incorrectly. While the χ²-function was fully minimized for the real data, it was evaluated on an inadequately large grid for the simulated data. As there were no errors in the χ²-values of the real data, the best-fit values are unaffected.

The correct p-values are listed in the table below. Since we observed fluctuations in the results between runs using 5000 random realizations, we increased the number of realizations to 250 000. The main conclusions of the paper are not affected by the changed numbers, because the main result of this method – that there is no evidence for a backside infall behind the Shapley Supercluster – remains the same. The higher p-value in the third redshift bin (0.045 <z < 0.06) does not contradict this observation.

We would like to thank Jeppe Trøst Nielsen for bringing this error to our attention and confirming the corrected numbers.

Table 1

Reconstructed directions (in Galactic coordinates) and corrected p-values of maximum anisotropy according to a dipole fit in different redshift bins for the Union2 and SNfactory datasets and their combination.

References

Feindt, U., Kerschhaggl, M., Kowalski, M., et al. 2013, A&A, 560, A90 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]

© ESO, 2015

All Tables

Table 1

Reconstructed directions (in Galactic coordinates) and corrected p-values of maximum anisotropy according to a dipole fit in different redshift bins for the Union2 and SNfactory datasets and their combination.

In the text

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[1] Feindt, U., Kerschhaggl, M., Kowalski, M., et al. 2013, A&A, 560, A90 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]